arXiv subjects

J. L. Morales Ortiz

Publications and source records attributed to J. L. Morales Ortiz.

3 recordsLinked to original sources

arXiv2026

A Study of HH 270 with the James Webb Space Telescope

We present a study of the Herbig-Haro object HH 270 based on observations from the James Webb Space Telescope (JWST), Subaru Telescope, and Atacama Large Millimeter/submillimeter Array (ALMA). High-resolution infrared images of H$_2$ and CO were obtained with the NIRCam instrument (JWST) using the F212N (2.12 $μ$m) and F460M (4.60 $μ$m) filters, revealing a previously unseen collimated protostellar jet closer to the source, in addition to the very well defined bipolar cavities carved by the outflow. Newly identified knots associated with the jet were also detected. Ground-based optical images in the H$α$ (660 nm) emission line, alongside millimeter spectral observations of the (2-1) transition of $^{12}$CO, $^{13}$CO, and C$^{18}$O, further enrich the analysis. The Subaru images show a connection between the optical outflow in H$α$ and the protostellar jet observed in the infrared. ALMA CO observations trace the kinematics of the entrained molecular gas in the protostellar outflow and reveal the dense, slow-moving material distributed around the driving source, HH270VLA1. These multi-wavelength observations show evidence of the interaction between the shock-excited jet emission and the molecular outflow seen at optical, infrared and radio wavelengths, which provides a detailed view of the complex structure and dynamics of HH 270.

astro-ph.SR↗

arXiv2025

HH 270/110 as a jet/shear layer interaction

New observations obtained with JWST of the proto-stellar HH~270 jet and the "deflected" HH 110 system, show that HH 110 has a morphology of a series of distorted working surfaces. These working surfaces appear to be "deflected versions" of the heads of the incident, HH 270 jet. We compute a series of 3D numerical simulations, in which we explore the possible parameters of a shearing environment that could give origin to the deflection of HH 270 into the HH 110 flow. We find that we need a quite high sideways velocity for the streaming environment (of ~30km/s) in order to produce the complex structure observed in HH 110. This high velocity would be possible in an environment which has been strongly perturbed by the passage of other outflows.

astro-ph.SR↗

arXiv2014

Ionization toward the high-mass star-forming region NGC 6334 I

Context. Ionization plays a central role in the gas-phase chemistry of molecular clouds. Since ions are coupled with magnetic fields, which can in turn counteract gravitational collapse, it is of paramount importance to measure their abundance in star-forming regions. Aims. We use spectral line observations of the high-mass star-forming region NGC 6334 I to derive the abundance of two of the most abundant molecular ions, HCO+ and N2H+, and consequently, the cosmic ray ionization rate. In addition, the line profiles provide information about the kinematics of this region. Methods. We present high-resolution spectral line observations conducted with the HIFI instrument on board the Herschel Space Observatory of the rotational transitions with Jup > 5 of the molecular species C17O, C18O, HCO+, H13CO+, and N2H+. Results. The HCO+ and N2H+ line profiles display a redshifted asymmetry consistent with a region of expanding gas. We identify two emission components in the spectra, each with a different excitation, associated with the envelope of NGC 6334 I. The physical parameters obtained for the envelope are in agreement with previous models of the radial structure of NGC 6334 I based on submillimeter continuum observations. Based on our new Herschel/HIFI observations, combined with the predictions from a chemical model, we derive a cosmic ray ionization rate that is an order of magnitude higher than the canonical value of 10^(-17) s-1. Conclusions. We find evidence of an expansion of the envelope surrounding the hot core of NGC 6334 I, which is mainly driven by thermal pressure from the hot ionized gas in the region. The ionization rate seems to be dominated by cosmic rays originating from outside the source, although X-ray emission from the NGC 6334 I core could contribute to the ionization in the inner part of the envelope.

astro-ph.GA↗